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09.09.2026 16:43
Research results, Scientific Publications

Discontinuity and disorder: explaining the luminosity bump in evolved stars

Main figure: a close-up of the bump with the luminosity maximum and minimum (Lmax and Lmin) indicated. The specific entropy at the surface is shown by the dashed light blue line and the axis on the right.
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Main figure: a close-up of the bump with the luminosity maximum and minimum (Lmax and Lmin) indicated. The specific entropy at the surface is shown by the dashed light blue line and the axis on the right. | Copyright: Saskia Hekker | Download

Towards the end of their lives, low-mass stars undergo an abrupt dip in their brightness, also known as the luminosity bump. Whereas the endpoint of this bump is well-understood, its onset has remained elusive. Now, in a paper published by The Astrophysical Journal Letters, Saskia Hekker, leader of the Theory and Observations of Stars group at the Heidelberg Institute for Theoretical Studies (HITS), finds that entropy is the key driver of the bump.

Towards the end of their lives, low-mass stars undergo an abrupt dip in their brightness, also known as the luminosity bump. Whereas the endpoint of this bump is well-understood, its onset has remained elusive. Now, in a paper published by The Astrophysical Journal Letters, Saskia Hekker, leader of the Theory and Observations of Stars group at the Heidelberg Institute for Theoretical Studies (HITS), finds that entropy is the key driver of the bump.

In observations and stellar evolution models alike, low-mass stars moving on the red-giant branch undergo a phenomenon known as the red-giant-branch bump, during which they temporarily experience a decrease in luminosity, where an increase would be expected. This confounding phenomenon has been investigated in Saskia Hekker’s latest research, wherein she demonstrates that the answer might be entropy, a measure of disorder. This process is usually precipitated by a discontinuity in the chemical composition of a star, emerging at the bottom of the convective stellar envelope, i.e. a star’s outer layers. In the course of evolution, the discontinuity moves to deeper layers with different temperatures and pressures, changing the entropy. This causes the star’s luminosity to decrease, thus defining the onset of the bump. “This succinct explanation of the onset of the bump, is the first quantitative description proposed so far,” says Hekker.

What does this mean for astrophysics?

Hekker’s research is the first of its kind and begins to answer a long-standing question in the history of astrophysics. According to Hekker, describing the mechanism behind the bump in this new way will provide key insights for the usage of the bump as an anchor point in stellar evolution theory.

Media contact:

Angela Michel
Head of Communications
Heidelberg Institute for Theoretical Studies (HITS)
+49 (0)6221 533 329
angela.michel@h-its.org

Wissenschaftlicher Ansprechpartner:
Prof. dr. ir. Saskia Hekker
Group Leader Theory and Observations of Stars group
Heidelberg Institute for Theoretical Studies (HITS)
https://www.h-its.org/people/prof-dr-saskia-hekker/

Professor of Astrophysics
Heidelberg University

Originalpublikation:
https://doi.org/10.3847/2041-8213/ae9ff0

Weitere Informationen:
https://www.h-its.org/2026/09/09/tos-luminosity-bump/

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